1.5-m - October 2001

General reduction notes for 1.5m f/13.5 data
CTIO 1.5m optical data (October 2001)

GENERAL REDUCTION NOTES for 1.5m f/13.5 data

for 1.5m f/13.5 data

gain=2

The data I reduced were taken on 2-3 Oct 2001. I reduced them to [OTZF] and to photometry.

PRELIMINARIES

1. Load data from tape. I used a directory called:

20011002/t60

Added this to loginuser.cl

#
set t20011002 = /uw54/nick/sn/20011002/t60/

and .daophot
#
setenv t20011002 /uw54/nick/sn/20011002/t60
alias t20011002 "cd $t20011002"

2. Copy over setup files (including the *.opt,*.clb files) from

copy /uw50/nick/daophot/optfiles/t60/f135/* .
cl < setup

3. Create data directory to copy all unwanted data

mkdir data

4. Run:

hedit *.imh OBSERVAT "CTIO" add+ up+ ver-
setjd *.imh
setairmass *.imh

5. Make the *.inf file

del in*,junk*
files obj*.imh > in1
hsel @in1 $I,filters,utmiddle,airmass,exptime,hjd,title,ha yes > junk.dat

!$myprog/prog3a junk.dat
0
t20011002
/uw50/nick/daophot/irafstuff/filters_t60.dat

CCD REDUCTIONS

If the data are not reduced, do so now.

1. Combine the zeros. Check first with nstat to see if there are any bad ones:

nstat zero*.imh

zerocomb zero*.imh combine="average" reject="minmax" nlow=0 nhigh=1
quadpr Zero

2. Reduce the spectral flats, dome flats, focus frames, and object frames to [OTZ]

quadpr sflat*.imh,dflat*.imh,focus*.imh,obj*.imh flatcor-

3. Create the shutter images

copy /uw50/nick/nickcl/shut? .

Make sure that the numbers in shut1 correspond to the dome exptime (20s).

imcomb focus* test1 comb=med reject=none
imcomb dflat0* test2 comb=med reject=none

The shutter error went from 0.065 in the corners to 0.085 in the center

cl < shut1
cl < shut2

4. Correct the short exposures with the shutter corrections.

shutcor sflat*.imh
cl < scor.cl
shutcor obj*.imh
cl < scor.cl

Shutcor will create a file called scor.cl which you run. Shutcor is slow.

5. Combine the twilight skies. You can use flatcomb, but I prefer to first separate the images by filter, look at the images and throw out the bad ones, and then combine.

fcomb sflat*.imh

This creates files called in_r, etc.

flatcomb @in_b comb=median reject=minmax nlow=0 nhigh=1
flatcomb @in_u comb=median reject=minmax nlow=0 nhigh=1
flatcomb @in_v comb=median reject=minmax nlow=0 nhigh=1
flatcomb @in_r comb=median reject=minmax nlow=0 nhigh=1
flatcomb @in_i comb=median reject=minmax nlow=0 nhigh=1
flatcomb @in_z comb=median reject=minmax nlow=0 nhigh=1

6. Now process the data to [OTZF]

quadpr obj*.imh

7. Make sure the data have been corrected for short exposures.

DAOPHOT

Make sure you have the *.opt files. Make sure the daophot.opt file has the right gain and readnoise.

daophot.opt:

photo.opt:

allstar.opt:

allframe.opt:

1. Measure the FWHM as:

del junk.dat
yaloshift @in1

etc.
Then run

!$myprog/prog39 junk.dat

This outputs fwhm.dat and fwhm1.dat. Use fwhm1.dat.

3. If you have standards, run BFIND2, using thresh about 10 for the bright stars. For SN data, run BYALO.

This will do BPASS2 and FINAL2. Use threshold of 5. For most f/13.5 data you can use a var = 1

If you use BPASS2 alone, edit the psf using:

!$myprog/prog11a r042 0.1

Lower the factor of 0.1 to about 0.07 for most frames.

Use dals for editing the psf stars. Often the center of a galaxy gets included in the psf.

If the SN or an important star was missed, run addals to add the object by hand.

Run FINAL2 to make the final psf phot and aperture files.

A note: DAOPHOT and all the programs identify stars by the x,y positions except in the case of making the psf. The psf is made from the file *.lst, and the stars here are identfied by the star name, not xy. If you change or add stars to the lst file, you must be sure that these names are the same as in the *.als files.

If you need to do ALLFRAME because the object is very weak, do:

a. make a *.mag file using DAOMASTER. Use 1 0.5 2 for input
b. renumber the *.mag stars using DAOPHOT
c. run BALLFRAME
d. run the following program to copy over the *.alf to *.als files
!$myprog/prog45 r055
e. make sure the *.mch file is pointing to the *.als data
f. run DAOMASTER to update the *.tfr file
!/uw50/nick/daophot/perl/daomaster.pl r032.mch

4. If you are doing aperture phot, make the *.lis file as ls -1 *.ap > feb04.lis.

The *.lis file should have the same number of lines as the *.inf file. You can check this as wc feb04.lib feb04.inf

ls -1 *ap > t20011002.lis

A note on file names. The following files should have the same name: *.inf, *.lis, *.obs, *.tfm, *.clb. It also helps to call the directory by that name also. For instance, if there are 5 nights, the third night would be in directory n3, and the following files would be created in directory n3: n3.inf, n3.lis, n3.obs, n3.tfm and n3.clb.

5. Then run DAOGROW.

I used 3 unknowns. Last 2 are 0.9 and 0. I used 0.03mag error limits. This produces *.tot files and a summary file *.gro. You can run "sm" at this point to see the growth curves. The command "see n3" will plot up 5 curves that represent the full range of  seeing. The command "gro obj100" etc will plot the growth curves.

If you need to rerun DAOGROW, run deldaogrow first.

6. Run DAOMATCH and DAOMASTER to make the tables for each field. This produces *.mch files for each field. To do this:

Use yalocenter to make a junk file with shifts and run the following program. Put "als" or "tot" as needed.

!$myprog/prog52b junk.dat als

This asks if you want to run daomaster. Do it.

!/uw50/nick/daophot/perl/daomaster.pl r032.mch

7. Display each first image in the *.mch files. Run the iraf task "fetch" and then the fortran task "fetch" to make the *.fet files.

The IRAF fetch inputs either an "a" key or an "x" key. Use the "a" key if the object looks like it can be centered. If the object is near a bad pix, use the "x" key.

8. Now, if you are doing standards, enter the data into COLLECT. Use prog43 to speed things up.

!$myprog/prog43 obj100

9. Now you run CCDSTD to get the transformations.

This produces *.rsd files which you can plot with sm. Use "resids highz99r" and "resids highz99i" which inputs the data.

t20011002.tfm:
M1=I1+I2
M2=I1
M3=I1-I3
M4=I1-I4
M5=I1+I2+I5
I1=M2
I2=M1-M2
I3=M2-M3
I4=M2-M4
I5=M5-M1
O1 = M1 + A0 + A1*I2 + A2*X + A3*T
O2 = M2 + B0 + B1*I2 + B2*X + B3*T
O3 = M3 + C0 + C1*I3 + C2*X + C3*T
O4 = M4 + D0 + D1*I4 + D2*X + D3*T
O5 = M5 + E0 + E1*I5 + E2*X + E3*T
A3=0. m:b,v,r,i,u
B3=0. i:V,B-V,V-R,V-I,U-B
C3=0.
D3=0.
E3=0.

10. The output of CCDSTD is a text file called *.clb. This is the final calibration file for the night.

If I have more than one night, at this point I reduce all nights through CCDSTD and average the color terms together. I then used the averaged terms and rerun CCDSTD.

11. Run CCDAVE to get the final library file, called *.net. CCDAVE is a very powerful program.

You can input multiple nights. Suppose you have 3 nights - n1,n2,n3. You then go to the directory which has n1,n2, and n3 and run CCDAVE. Input the files n1/n1.inf, n2/n2.inf, etc. The output of CCDAVE will average the results across all nights. The library file is *.net, and the individual measurements are

*.ave. Look at the *.ave file to get a feel for how well the data repeats.

Copy the *.ave,*.net,*.clb files to /uw50/nick/daophot/clbfiles and include one explanatory file.

12. Once you have the *.net file, run REDUCE. For reduce, you need the

*.inf
*.tfr
E
*.net
*.fet

to run. The output will be *.fnl, and the zero-point calculation is given in *.zer. You can id the stars quickly by displaying the master image (usually the first file in the *.mch file or the first line in the *.tfr file) and running the IRAF script fnl.cl

Note that the *.tfr file MUST be made at the last minute. To be safe, you may want to run daomaster.pl to make a fresh copy of the *.tfr file just in case.

You should create a shortened image for the master frame for the *.fnl file, in case you are archiving the data.
 

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